Resolving the Inner Arcsecond of the RY Tau Jet with HST

Abstract

Abstract Faint X-ray emission from hot plasma (T x > 106 K) has been detected extending outward a few arcseconds along the optically delineated jets of some classical T Tauri stars including RY Tau. The mechanism and location where the jets are heated to X-ray temperatures are unknown. We present high spatial resolution Hubble Space Telescope (HST) far-ultraviolet long-slit observations of RY Tau with the slit aligned along the jet. The primary objective was to search for C iv emission from warm plasma at T C iv ∼ 105 K within the inner jet (<1″) that cannot be fully resolved by X-ray telescopes. Spatially resolved C iv emission is detected in the blueshifted jet extending outward from the star to 1″ and in the redshifted jet out to 0.″5. C iv line centroid shifts give a radial velocity in the blueshifted jet of −136 ± 10 km s−1 at an offset of 0.″29 (39 au) and deceleration outward is detected. The deprojected jet speed is subject to uncertainties in the jet inclination, but values ≳200 km s−1 are likely. The mass-loss rate in the blueshifted jet is at least M ˙ jet , blue = 2.3 × 10 − 9 M ⊙ yr−1, consistent with optical determinations. We use the HST data along with optically determined jet morphology to place meaningful constraints on candidate jet-heating models including a hot-launch model in which the jet is heated near the base to X-ray temperatures by an unspecified (but probably magnetic) process, and downstream heating from shocks or a putative jet magnetic field.